2019A&A...631A.108K


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.23CEST22:41:48

2019A&A...631A.108K - Astronomy and Astrophysics, volume 631A, 108-108 (2019/11-1)

VLTI/PIONIER survey of disks around post-AGB binaries. Dust sublimation physics rules.

KLUSKA J., VAN WINCKEL H., HILLEN M., BERGER J.-P., KAMATH D., LE BOUQUIN J.-B. and MIN M.

Abstract (from CDS):


Context. Post-asymptotic giant branch (AGB) binaries are surrounded by circumbinary disks of gas and dust that are similar to protoplanetary disks found around young stars.
Aims. We aim to understand the structure of these disks and identify the physical phenomena at play in their very inner regions. We want to understand the disk-binary interaction and to further investigate the comparison with protoplanetary disks.
Methods. We conducted an interferometric snapshot survey of 23 post-AGB binaries in the near-infrared (H-band) using VLTI/PIONIER. We fit the multi-wavelength visibilities and closure phases with purely geometrical models with an increasing complexity (including two point-sources, an azimuthally modulated ring, and an over-resolved flux) in order to retrieve the sizes, temperatures, and flux ratios of the different components.
Results. All sources are resolved and the different components contributing to the H-band flux are dissected. The environment of these targets is very complex: 13/23 targets need models with thirteen or more parameters to fit the data. We find that the inner disk rims follow and extend the size-luminosity relation established for disks around young stars with an offset toward larger sizes. The measured temperature of the near-infrared circumstellar emission of post-AGB binaries is lower (Tsub∼1200K) than for young stars, which is probably due to a different dust mineralogy and/or gas density in the dust sublimation region.
Conclusions. The dusty inner rims of the circumbinary disks around post-AGB binaries are ruled by dust sublimation physics. Additionally a significant amount of the circumstellar H-band flux is over-resolved (more than 10% of the non-stellar flux is over-resolved in 14 targets). This hints that a source of unknown origin, either a disk structure or outflow. The amount of over-resolved flux is larger than around young stars. Due to the complexity of these targets, interferometric imaging is a necessary tool to reveal the interacting inner regions in a model-independent way.

Abstract Copyright: © ESO 2019

Journal keyword(s): stars: AGB and post-AGB - techniques: high angular resolution - techniques: interferometric - binaries: general - circumstellar matter - protoplanetary disks

VizieR on-line data: <Available at CDS (J/A+A/631/A108): fitparam.dat>

Simbad objects: 25

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Number of rows : 25

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* AY Lep pA* 05 22 59.4223189375 -20 32 53.046745853   10.52 9.48     ~ 23 0
2 V* PS Gem pA* 07 03 39.6306725638 +10 46 13.076555664   7.76 7.37     A0 106 0
3 V* U Mon RV* 07 30 47.4734611972 -09 46 36.788534824 8.22 7.00 5.82     G8/K0Ib/II 193 0
4 CD-44 4961 pA* 08 56 14.1790943091 -44 43 10.710041643   10.55 9.176     F3e 57 1
5 V* IW Car RV* 09 26 53.3043066360 -63 37 48.939300156   9.07 7.90     F7/8 87 0
6 V* V494 Vel LP* 09 41 51.9354310226 -47 46 57.812002542   12.28 10.45     ~ 1 0
7 IRAS 09400-4733 * 09 41 53.1591976979 -47 47 08.986190299           M0 6 0
8 HD 89353 pA* 10 18 07.5892879413 -28 59 31.194541133   5.76 5.53     B9.5Ib/II 287 0
9 V* V709 Car pA* 10 19 16.8819372679 -57 19 25.874710095   12.71 11.28     G8Ia-0 14 0
10 HD 93662 pA* 10 47 38.3963525198 -57 28 02.673468362   7.954 6.248     K5/M0(III) 31 0
11 V* V802 Car pA* 11 02 04.3151180751 -62 09 42.834842337   9.57 8.90 9.38   F2III 49 0
12 V* RU Cen RV* 12 09 23.8147186123 -45 25 34.813401164   9.81 8.70     G1Ie 87 0
13 V* SX Cen RV* 12 21 12.5740806517 -49 12 41.059392756   10.11 9.60     B5III 66 0
14 HD 108015 pA* 12 24 53.5038403586 -47 09 07.498401573   8.379 7.96     F3/5Ib/II 56 0
15 V* EN TrA pA* 14 57 00.6830179855 -68 50 22.901317885   9.42 8.70     F2Ib 65 0
16 IRAS 15469-5311 pA* 15 50 43.8045787663 -53 20 43.254393089   12.03 10.66     F3 22 0
17 V* NN Ser No* 15 52 56.1202658103 +12 54 44.432043501     16.51     DAO1+M4 232 0
18 CD-48 11445 pA* 17 07 36.6576312333 -48 19 08.476517172   12.33 10.55     G2p(R) 29 0
19 V* LR Sco RV* 17 27 53.6264684155 -43 50 46.286212209   11.45 10.37     G0I 30 0
20 V* AI Sco RV* 17 56 18.5761406960 -33 48 43.261703840   10.99 9.98     G5 44 0
21 V* V2053 Oph pA* 18 14 49.3842596707 +05 12 55.717076925   11.75 10.28     C 39 0
22 V* AC Her pA* 18 30 16.2374666779 +21 52 00.618442618 8.00 7.79 7.01     F4Ibp 316 0
23 V* R Sct RV* 18 47 28.9509385830 -05 42 18.537825839 8.30 6.67 5.20 4.14 3.37 K4/5pec 295 0
24 BD+03 3950 RV* 19 15 01.1800400072 +03 48 42.640112771   11.16 10.37     F8 32 0
25 V* HM Aqr pA* 22 35 27.5256072315 -17 15 26.885199823 9.31 9.08 8.90     A0III 100 0

    Equat.    Gal    SGal    Ecl

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2020.09.23-22:41:48

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